Palestrante
Descrição
Cosmic rays are charged particles propagating through the universe and reaching the Earth with different energy and composition. Several studies are being carried out to find the sources of this radiation. One possible source of galactic cosmic rays are the so-called PeVatrons, which can accelerate these particles to an energy of 10¹⁵ eV. This energy band in the cosmic ray spectrum is called the “knee”, characterized by a change in the spectral index. To study PeVatrons, the relationship between gamma-rays in the energy range from GeV to TeV and cosmic rays up to PeV is observed. The LHAASO observatory has discovered a population of PeVatrons near the galactic center whose photons reach an energy of up to 1.4 PeV. In this work, two of these PeVatrons cataloged by LHAASO will be presented, both of which have two pulsars in their region as possible sources of acceleration of the detected radiation. LHAASO J1825-1326 with pulsars PSR J1826-1334 and PSR J1826-1256 and LHAASO J1839-0545 with pulsars PSR J1837-0604 and J1838-0537. We have performed simulations of cosmic ray propagation and interaction in the galaxy using the spin-down model with the GALPROP software for the four pulsars. We will present the gamma-ray results from these simulations and compare them with data from different observatories. We will also show a spectral energy distribution of pulsars analyzed using gamma-ray observations from CTA simulations with the software Gammapy. The results show a contribution of gamma rays from these sources to observatory data at different energies and possible future observations in these regions by the CTA observatory.
